NGC 7496

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NGC 7496
Hubble Goes Galactic Birdwatching (potw2222a).jpg
NGC 7496 by the Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Grus
Right ascension 23h 09m 47.3s [1]
Declination −43° 25′ 40.6″ [1]
Redshift 0.005500 ± 0.000018 [1]
Heliocentric radial velocity 1,649 ± 5 km/s [1]
Distance 61 Mly (18.7 Mpc) [2]
Apparent magnitude  (V)11.1
Characteristics
Type (R':)SB(rs)bc [1]
Apparent size  (V)3.3′ × 3.0′ [1]
Notable features Seyfert galaxy, starburst galaxy
Other designations
ESO 291- G001, VV 771, MCG -07-47-020, PGC 70588 [1]

NGC 7496 is a barred spiral galaxy located in the constellation Grus. It is located at a distance of about 60 million light-years from Earth, which, given its apparent dimensions, means that it is 75,000 light years across. It was discovered by John Herschel on September 5, 1834. [3] It is a type 2 Seyfert galaxy with high star formation rate around the nucleus. [4]

Contents

Characteristics

The nucleus of the galaxy has been found to be active and it has been categorised as a type 2 Seyfert galaxy. The nucleus has fairly strong emission lines in the optical wavelengths and an intense source of ultraviolet radiation. The spectrum also revealed the presence of an HII region in the nucleus, indicating the presence of young hot stars. The nucleus is also a source of radio waves. [5] The most accepted theory for the energy source of active galactic nuclei is the presence of an accretion disk around a supermassive black hole.

NGC 7496 was one of the first galaxies to be examined by the James Webb Space Telescope, in June 2022, as part of the Physics at High Angular resolution in Nearby GalaxieS (PHANGS)–JWST survey, whose goal was to study star formation and the interstellar medium in nearby galaxies. [6] The mid infrared images revealed filaments and cavities created by the stellar wind of young stars. Imaging of 3.3 μm polycyclic aromatic hydrocarbons (PAH) emission, which is caused the ultraviolet radiation being reprossesed by dust, revealed the presence of 67 candidate star clusters embedded in dust. The age of these clusters was estimated to be less than 2 million years while their mass was estimated to be 104–105 M☉. Their location was also correlated with H-alpha and CO(2–1) emission. [2]

Clumpy ultraviolet emission has been observed from the spiral arms of the galaxy. Massive stellar complexes are present in the north arm and regions with young stellar complexes are present in the end of both arms. The age of the stars in these complexes is estimated to be less than 200 million years. Photometry in various wavelengths indicates that there is very cold dust in the galaxy. [7]

Nearby galaxies

NGC 7496 is a member of the NGC 7582 galaxy group. [8] Other members of the group include NGC 7552, NGC 7582, NGC 7590, and NGC 7599, which are also known as the Grus Quartet, [9] NGC 7531, NGC 7632, and IC 5325. [8] This group, along with the group centred around IC 1459 form the Grus cloud, a region of elevated galaxy density. The Grus cloud, along with the nearby Pavo-Indus cloud, lies between the Local Supercluster and Pavo–Indus Supercluster. [10]

See also

Related Research Articles

<span class="mw-page-title-main">Seyfert galaxy</span> Class of active galaxies with very bright nuclei

Seyfert galaxies are one of the two largest groups of active galaxies, along with quasars. They have quasar-like nuclei with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, their host galaxies are clearly detectable.

<span class="mw-page-title-main">NGC 1087</span> Galaxy in the constellation Cetus

NGC 1087 is an intermediate spiral galaxy in Cetus. The central bar/core is very small with many irregular features in the surrounding disk of material. With the many strange features of NGC 1087, its true nature is still uncertain. It has an extremely small nucleus and a very short stellar bar. Unlike most barred galaxies, the bar apparently has some new star-formation taking place. There is a multiple spiral structure defined more by the dust lanes than by luminous matter. Overall, the disc has a very low surface brightness. Even though it appears close to another galaxy, these two galaxies are not interacting and should be considered isolated from one another.

<span class="mw-page-title-main">NGC 1672</span> Galaxy in the constellation Dorado

NGC 1672 is a barred spiral galaxy located in the constellation Dorado. It was discovered by the astronomer James Dunlop on November 5, 1826. It was originally unclear whether it was a member of the Dorado Group, with some sources finding it to be a member and other sources rejecting its membership. However, recent tip of the red-giant branch (TRGB) measurements indicate that NGC 1672 is located at the same distance as other members, suggesting it is indeed a member of the Dorado Group.

<span class="mw-page-title-main">NGC 7319</span> Galaxy in the constellation Pegasus

NGC 7319 is a highly distorted barred spiral galaxy that is a member of the compact Stephan's Quintet group located in the constellation Pegasus, some 311 megalight-years distant from the Milky Way. The galaxy's arms, dust and gas have been highly disturbed as a result of the interaction with the other members of the Quintet. Nearly all of the neutral hydrogen has been stripped from this galaxy, most likely as a result of a collision with NGC 7320c some 100 million years ago. A pair of long, parallel tidal tails extend southward from NGC 7319 in the direction of NGC 7320c, and is undergoing star formation.

<span class="mw-page-title-main">Ionization cone</span> Astronomical phenomenon

Ionization cones are cones of ionized material extending from active galactic nuclei, predominantly observed in type II Seyfert galaxies. They are detected through their emission of electromagnetic radiation in the visible and infrared parts of the spectrum. The main method of observation is through spectroscopy, using spectral line analysis to measure the shape of the ionized region and the condition of the material such as temperature, density, composition, and degree of ionization.

<span class="mw-page-title-main">NGC 2835</span> Spiral galaxy in the constellation Hydra

NGC 2835 is an intermediate spiral galaxy located in the constellation Hydra. It is located at a distance of circa 35 million light years from Earth, which, given its apparent dimensions, means that NGC 2835 is about 65,000 light years across. It was discovered by Wilhelm Tempel on April 13, 1884. NGC 2835 is located only 18.5 degrees from the galactic plane.

<span class="mw-page-title-main">NGC 7213</span> Galaxy in the constellation Grus

NGC 7213 is a lenticular galaxy located in the constellation Grus. It is located at a distance of circa 70 million light-years from Earth, which, given its apparent dimensions, means that NGC 7213 is about 75,000 light-years across. It was discovered by John Herschel on September 30, 1834. It is an active galaxy with characteristics between a type I Seyfert galaxy and LINER.

<span class="mw-page-title-main">NGC 7130</span> Galaxy in the constellation Piscis Austrinus

NGC 7130 is a spiral galaxy located in the constellation Piscis Austrinus. It is located at a distance of about 220 million light years from Earth, which, given its apparent dimensions, means that NGC 7130 is about 100,000 light years across. It was discovered by John Herschel on September 25, 1834, and discovered independently by Lewis Swift on September 17, 1897. The location of the galaxy given in the New General Catalogue was off by 30 arcminutes in declination from the location of the galaxy.

<span class="mw-page-title-main">NGC 985</span> Ring galaxy in the constellation Cetus

NGC 985 is a ring galaxy in the constellation of Cetus. It is located about 550 million light years away from Earth, which means, given its apparent dimensions, that NGC 985 is approximately 160,000 light years across. It was discovered by Francis Leavenworth in 1886. It is a type 1 Seyfert galaxy.

<span class="mw-page-title-main">NGC 6951</span> Galaxy in the constellation Cepheus

NGC 6951 is a barred spiral galaxy located in the constellation Cepheus. It is located at a distance of about 75 million light-years from Earth, which, given its apparent dimensions, means that NGC 6951 is about 100,000 light-years across. It was discovered by Jérôme Eugène Coggia in 1877 and independently by Lewis Swift in 1878.

<span class="mw-page-title-main">NGC 3489</span> Galaxy in the constellation Leo

NGC 3489 is a lenticular galaxy located in the constellation Leo. It is located at a distance of about 30 million light years from Earth, which, given its apparent dimensions, means that NGC 3489 is about 30,000 light years across. It was discovered by William Herschel on April 8, 1784. NGC 3489 is a member of the Leo Group.

<span class="mw-page-title-main">NGC 4636</span> Galaxy in the constellation Virgo

NGC 4636 is an elliptical galaxy located in the constellation Virgo. It is a member of the NGC 4753 Group of galaxies, which is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster. It is located at a distance of about 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4636 is about 105,000 light years across.

<span class="mw-page-title-main">NGC 5846</span> Galaxy in the constellation Virgo

NGC 5846 is an elliptical galaxy located in the constellation Virgo. It is located at a distance of circa 90 million light years from Earth, which, given its apparent dimensions, means that NGC 5846 is about 110,000 light years across. It was discovered by William Herschel on February 24, 1786. It lies near 110 Virginis and is part of the Herschel 400 Catalogue. It is a member of the NGC 5846 Group of galaxies, itself one of the Virgo III Groups strung out to the east of the Virgo Supercluster of galaxies.

<span class="mw-page-title-main">NGC 3665</span> Galaxy in the constellation Ursa Major

NGC 3665 is a lenticular galaxy located in the constellation Ursa Major. It is located at a distance of circa 85 million light-years from Earth, which, given its apparent dimensions, means that NGC 3665 is about 85,000 light years across. It was discovered by William Herschel on March 23, 1789.

<span class="mw-page-title-main">NGC 7531</span> Galaxy in the constellation Grus

NGC 7531 is an intermediate spiral galaxy located in the constellation Grus. It is located at a distance of circa 70 million light-years from Earth, which, given its apparent dimensions, means that NGC 7531 is about 95,000 light years across. It was discovered by John Herschel on September 2, 1836.

<span class="mw-page-title-main">IC 1459</span> Elliptical galaxy in the constellation of Grus

IC 1459 is an elliptical galaxy located in the constellation Grus. It is located at a distance of circa 85 million light-years from Earth, which, given its apparent dimensions, means that IC 1459 is about 130,000 light-years across. It was discovered by Edward Emerson Barnard in 1892.

<span class="mw-page-title-main">NGC 4278</span> Galaxy in the constellation Coma Berenices

NGC 4278 is an elliptical galaxy located in the constellation Coma Berenices. It is located at a distance of circa 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4278 is about 65,000 light years across. It was discovered by William Herschel on March 13, 1785. NGC 4278 is part of the Herschel 400 Catalogue and can be found about one and 3/4 of a degree northwest of Gamma Comae Berenices even with a small telescope.

<span class="mw-page-title-main">NGC 7418</span> Galaxy in the constellation Grus

NGC 7418 is an intermediate spiral galaxy located in the constellation Grus. It is located at a distance of circa 60 million light-years from Earth, which, given its apparent dimensions, means that NGC 7418 is about 60,000 light-years across. It was discovered by John Herschel on August 30, 1834.

<span class="mw-page-title-main">NGC 5363</span> Galaxy in the constellation Virgo

NGC 5363 is a lenticular galaxy located in the constellation Virgo. It is located at a distance of circa 65 million light years from Earth, which, given its apparent dimensions, means that NGC 5363 is about 100,000 light years across. It was discovered by William Herschel on January 19, 1784. It is a member of the NGC 5364 Group of galaxies, itself one of the Virgo III Groups strung out to the east of the Virgo Supercluster of galaxies.

<span class="mw-page-title-main">NGC 680</span> Galaxy in the constellation Aries

NGC 680 is an elliptical galaxy located in the constellation Aries. It is located at a distance of circa 120 million light years from Earth, which, given its apparent dimensions, means that NGC 680 is about 100,000 light years across. It was discovered by William Herschel on September 15, 1784.

References

  1. 1 2 3 4 5 6 7 "NASA/IPAC Extragalactic Database". Results for NGC 7496. Retrieved 2019-01-18.
  2. 1 2 Rodríguez, M. Jimena; Lee, Janice C.; Whitmore, B. C.; Thilker, David A.; Maschmann, Daniel; Chandar, Rupali; Deger, Sinan; Boquien, Médéric; Dale, Daniel A.; Larson, Kirsten L.; Williams, Thomas G.; Kim, Hwihyun; Schinnerer, Eva; Rosolowsky, Erik; Leroy, Adam K.; Emsellem, Eric; Sandstrom, Karin M.; Kruijssen, J. M. Diederik; Grasha, Kathryn; Watkins, Elizabeth J.; Barnes, Ashley. T.; Sormani, Mattia C.; Kim, Jaeyeon; Anand, Gagandeep S.; Chevance, Mélanie; Bigiel, F.; Klessen, Ralf S.; Hassani, Hamid; Liu, Daizhong; Faesi, Christopher M.; Cao, Yixian; Belfiore, Francesco; Pessa, Ismael; Kreckel, Kathryn; Groves, Brent; Pety, Jérôme; Indebetouw, Rémy; Egorov, Oleg V.; Blanc, Guillermo A.; Saito, Toshiki; Hughes, Annie (1 February 2023). "PHANGS–JWST First Results: Dust-embedded Star Clusters in NGC 7496 Selected via 3.3 μm PAH Emission". The Astrophysical Journal Letters. 944 (2): L26. doi: 10.3847/2041-8213/aca653 .
  3. ↑ Seligman, Courtney. "NGC 7496 (= PGC 68165)". Celestial Atlas. Retrieved 19 November 2018.
  4. ↑ Schmitt, H. R.; Calzetti, D.; Armus, L.; Giavalisco, M.; Heckman, T. M.; Kennicutt, R. C. Jr.; Leitherer, C.; Meurer, G. R. (May 2006). "Multiwavelength Star Formation Indicators: Observations". The Astrophysical Journal Supplement Series. 164 (1): 52–80. arXiv: astro-ph/0602063 . doi: 10.1086/501529 .
  5. ↑ Kinney, A. L.; Bohlin, R. C.; Calzetti, D.; Panagia, N.; Wyse, Rosemary F. G. (May 1993). "An atlas of ultraviolet spectra of star-forming galaxies". The Astrophysical Journal Supplement Series. 86: 5. doi: 10.1086/191771 .
  6. ↑ Lee, Janice C.; Sandstrom, Karin M.; Leroy, Adam K.; Thilker, David A.; Schinnerer, Eva; Rosolowsky, Erik; Larson, Kirsten L.; Egorov, Oleg V.; Williams, Thomas G.; Schmidt, Judy; Emsellem, Eric; Anand, Gagandeep S.; Barnes, Ashley T.; Belfiore, Francesco; Bešlić, Ivana; Bigiel, Frank; Blanc, Guillermo A.; Bolatto, Alberto D.; Boquien, Médéric; Brok, Jakob den; Cao, Yixian; Chandar, Rupali; Chastenet, Jérémy; Chevance, Mélanie; Chiang, I-Da; Congiu, Enrico; Dale, Daniel A.; Deger, Sinan; Eibensteiner, Cosima; Faesi, Christopher M.; Glover, Simon C. O.; Grasha, Kathryn; Groves, Brent; Hassani, Hamid; Henny, Kiana F.; Henshaw, Jonathan D.; Hoyer, Nils; Hughes, Annie; Jeffreson, Sarah; Jiménez-Donaire, María J.; Kim, Jaeyeon; Kim, Hwihyun; Klessen, Ralf S.; Koch, Eric W.; Kreckel, Kathryn; Kruijssen, J. M. Diederik; Li, Jing; Liu, Daizhong; Lopez, Laura A.; Maschmann, Daniel; Chen, Ness Mayker; Meidt, Sharon E.; Murphy, Eric J.; Neumann, Justus; Neumayer, Nadine; Pan, Hsi-An; Pessa, Ismael; Pety, Jérôme; Querejeta, Miguel; Pinna, Francesca; Rodríguez, M. Jimena; Saito, Toshiki; Sánchez-Blázquez, Patricia; Santoro, Francesco; Sardone, Amy; Smith, Rowan J.; Sormani, Mattia C.; Scheuermann, Fabian; Stuber, Sophia K.; Sutter, Jessica; Sun, Jiayi; Teng, Yu-Hsuan; Treß, Robin G.; Usero, Antonio; Watkins, Elizabeth J.; Whitmore, Bradley C.; Razza, Alessandro (1 February 2023). "The PHANGS–JWST Treasury Survey: Star Formation, Feedback, and Dust Physics at High Angular Resolution in Nearby GalaxieS". The Astrophysical Journal Letters. 944 (2): L17. arXiv: 2212.02667 . doi: 10.3847/2041-8213/acaaae .
  7. ↑ Singh, Swapnil; Ashby, M L N; Vig, Sarita; Ghosh, S K; Jarrett, T; Crawford, T M; Malkan, Matthew A; Archipley, M; Vieira, J D (12 May 2021). "The cold dust content of the nearby galaxies IC 5325, NGC 7496, NGC 7590, and NGC 7599". Monthly Notices of the Royal Astronomical Society. 504 (3): 4143–4159. arXiv: 2104.06236 . doi: 10.1093/mnras/stab1048 .
  8. 1 2 Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z~ 0.01) Universe". Monthly Notices of the Royal Astronomical Society. 412 (4): 2498–2520. arXiv: 1011.6277 . Bibcode:2011MNRAS.412.2498M. doi:10.1111/j.1365-2966.2010.18071.x. S2CID   119194025. Archived from the original on 31 January 2016. Retrieved 20 January 2019.
  9. ↑ Bakich, Michael E. (2010). 1,001 Celestial Wonders to See Before You Die. New York, New York: Springer Science+Business Media, LLC. p. 334. Bibcode:2010ocws.book.....B. ISBN   978-1-4419-1777-5.
  10. ↑ Fouque, P.; Proust, D.; Quintana, H.; Ramirez, A.; Proust, D.; Quintana, H.; Ramirez, A. (1993). "Dynamics of the Pavo-Indus and Grus Clouds of Galaxies" (PDF). Astronomy and Astrophysics Supplement Series. 100 (3): 493–500. Bibcode:1993A&AS..100..493F.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  11. ↑ "NGC 7496 (MIRI Image)". www.esawebb.org. 16 February 2023. Retrieved 18 November 2023.
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